Speaker
Description
Rapid rotation and strong magnetic fields can reshape the dynamics, energetics, and multimessenger emission of core-collapse supernovae. We investigate these effects using three-dimensional magnetohydrodynamic simulations together with hydrodynamic control models.
Rotation alone modifies the protoneutron star structure, neutrino emission, post-shock dynamics, and the development of non-axisymmetric instabilities. Magnetic fields can alter this evolution further by redistributing angular momentum, extracting free energy from differential rotation, and reorganizing the flow into magnetically influenced outflows. These effects are reflected in the gravitational wave signal through rotational dynamics, protoneutron star oscillations, and large-scale asymmetries, while the neutrino signal traces changes in accretion geometry and remnant structure.
Interpreting these physical and multimessenger signatures also requires understanding how magnetic energy is processed within the simulations. Energy budget diagnostics suggest that part of the extracted magnetic energy is neither retained in the resolved magnetic field nor accounted for by the resolved channels of magnetic energy conversion and transport through Lorentz work and Poynting flux, but instead appears in a dissipation-like residual. Determining whether this residual reflects unresolved reconnection, numerical diffusion, or both is important for assessing magnetic field saturation, outflow power, energy conversion efficiency, and the connection between rotational energy loss and explosion energetics. We discuss how this uncertainty may affect the physical interpretation of the overall dynamics and the multimessenger predictions of global magnetorotational supernova simulations.